Non-Thermal Dark Matter from Moduli Decay. Bhaskar Dutta. Texas A&M University

Transcription

1 Non-Thermal Dark Matter rom Moduli Decay Bhaskar Dutta Texas A&M University Allahverdi, Dutta, Sinha, PRD87 (2013) , PRDD86 (2012) , PRD83 (2011) , PRD82 (2010) Allahverdi, Dutta, Mohapatra Sinha, PRL 111, (2013) Allahverdi, Cicoli, Dutta, Sinha, Phys. Rev. D 88, (2013) Allahverdi, Dutta, Phys.Rev. D88 (2013)

2 Outline Thermal and Non-thermal Dark Matter () Heavy Scalar/Moduli Decay and Baryogenesis rom the Decay o Heavy Scalar Direct Detection Model Examples Conclusion 2

3 Thermal Dark Matter Production o thermal : Non-relativistic Freeze-Out: Hubble expansion dominates over the interaction rate Dark Matter Content: reeze out v 310 v T 26 m 20 ~ ~ 2 Assuming : 2 cm 3 s m ~ 1 v m/t ~O(10-2 ) with m ~ O(100) GeV leads to the correct relic abundance 3

4 Thermal Dark Matter particle + Particle SM particles Annihilation Cross-section Rate: ann v Abundance: 1 ~ v ~ : SM particles; h, H, A: various Higgs, : SUSY particle We need v cm 3 s to satisy thermal requirement 4

5 Thermal Dark Matter Suitable Candidate: Weakly Interacting Massive Particle (WIMP) Typical in Physics beyond the SM (LSP, LKP, ) Most Common: Neutralino (SUSY Models) smaller annihilation cross-section Neutralino: Mixture o Wino, Higgsino and Bino Larger annihilation cross-section Larger/Smaller Annihilation Non-thermal Models 5

6 Thermal, Non-thermal ann v can be larger or smaller than the thermal average value Gamma-rays constraints: Dwar spheroidals, Galactic center Thermal 27% Large Crosssection is constrained ann v o : smaller than the thermal value Geringer-Sameth, Koushiappas, Phys. Rev. Lett. 107, (2011) Hooper, Kelso, Queiroz, Astropart.Phys. 46 (2013) 55 6

7 Non-Thermal : dierent rom thermal average, i.e., 1 26% ~ Non-thermal can be a solution v v ann rom the decay o heavy scalar ield, e.g., Moduli decay [Moduli : heavy scalar ields gravitationally coupled to matter] Decay o moduli/heavy ield occurs at: T r ~ c 1/ 2 m 100TeV 3/ 2 (5MeV) For T r <T : Non-thermal dark matter Abundance o decay products T r ~ MeV : Not allowed by BBN Y 3T r 4m Barrow, 82; Kamionkowski,Turner, 90; Gelmini, Gondolo, Soldatenko, Yaguna, 07 Allahverdi, Dutta, Sinha, 09, 10, 11, 12, 13; Acharya,Kane, Kumar,Watson, 09, 10 7

8 Beneit Dark o Matter Non-Thermal rom abundance: For T r < T, larger annihilation cross-section is needed or 26% ann v ann v th T T r r For T r << T, Yield Y is small enough ( m ) will be produced without any need o annihilation Outcome: 3T Large and small annihilation cross-section rom models are okay We may not need any annihilation Since other particles, abundance (or T r << T ): The Baryon and the abundance are correlated ~ Allahverdi, Dutta, Sinha, Phys.Rev. D83 (2011) ; 8

9 Dark Matter rom production rom the decay Y = n s min.[ n s obs v v Th T T r, Y Br ] Where 1GeV ; m n v th 310 cm s s obs Y 3T 4m r 0.9 cm M p Br -> is the branching ratio or R parity odd particles which are responsible or generating candidates 9

10 abundance Dark Matter rom n s n s 1. First term on the RHS is the annihilation scenario Requires: th T ann v min.[ ann v T r th Since T r < T, we need annv annv wino/higgsino Gamma-rays constraints: Dwar spheroidals, Galactic center M > 40 GeV, T < 30 T r T r > 70 MeV obs v v Th T T r, Y Br ] 2. Second term on the RHS is the branching scenario Can accommodate large and small annihilation cross-sections Bino/Wino/Higgsino are all ok Y is small to prevent the Br rom becoming too small Allahverdi, Dutta, Sinha, Phys.Rev. D83 (2011) ; 10

11 Dark Matter rom Branching scenario solves the coincidence problem abundance in this model: n Y Br Y ~ s Baryon abundance in this model: n s B Y Br B BR B ~ easy to satisy or baryogenesis, (one loop actor) ~ b 1 m Y Br Y Br B 1 m Br Br B 1 5 =r/r c ; r=mn For m ~ 5 m B, n B ~ n BR B ~ BR The abundance and Baryon asymmetry are mostly saturated by Y, Brs contribute the remaining not much particle physics uncertainty

12 Dark Matter rom So Far Thermal gets diluted i T r < T ~ m /20 ~ O(10) GeV Axionic gets diluted i T r < L QCD ~ 200 MeV Baryon asymmetry gets diluted i produced beore decay Non-thermal Production rom decay Annihilation scenario or T r close to T production with large cross-section: Wino/Higgsino Branching scenario or smaller T r (annihilation cross-section does not matter) New mechanism or Baryon Asymmetry is needed 12

13 Dark Matter & Baryogenesis rom N ~ N W extra i N u c i X X, ' ij X d c i d c j X M : SM singlet; : Color triplet, hypercharge 4/3 N ermions and X scalars and their SUSY partners R parity conserved : can be the candidate (spin 0) with small mass and large spin-independent cross-section [ Allahverdi, Dutta, Mohapatra, Sinha, PRL 111, (2013)] X X M 2 N N Baryogenesis rom decays o X, X or N 13

14 Baryogenesis rom From X decay Typically, 1,2 is O(10-2 ) or CP violating phase O(1) and ~O(1) 14

15 Dark Matter Candidates: Direct Detection Direct detection scattering cross-section: N ~ Suppose: N ~ ~ N, c i N ~ Xu i Scatters o a quark via s-channel exchange o X N or ~ is the particle (spin-0) For i ~1, M x ~ 1 TeV, I N (spin ½) is, M N ~m p (to prevent N decay and p-decay), N-p is cm 2 (SI) and cm 2 (SD)

16 Non-Thermal LHC Final states at the LHC New Particles: Heavy colored states: SM Singlet: LHC signals: new colored states -spin 0- are pair produced high E T our jets in the inal states new colored states spin ½- are pair produced, high E T our jets +missing energy [via cascade decays into squarks etc] X, Distinguishing Feature: 4 high E T jets and 4 high E T jets + missing energy X N 16

17 Model Example I is a modulus: Two typical problems or moduli decay Gravitino Problem: [Endo,Hamaguchi,Takahashi][Nakamura,Yamaguchi] I m 3/2 <50 TeV Gravitino decays ater the BBN m >m 3/2 can lead to overproduction: decay into gravitinos [Cicoli,Conlon,Quevedo][Higaki,Takahashi] Model example: [Based on: R. Blumenhagen, J. P. Conlon, S. Krippendor, S. Moster and F. Quevedo] Large Volume Scenario: Type IIB LVS models Lightest modulus mass m <m 3/2 ; m sot ~ m 3/2. =m 3/2 /M p <<1 Both branching and annihilation scenarios can be accommodated Dominant decay modes o the moduli involve the gauge Bosons (branching scenario) [Allahverdi, Cicoli, Dutta, Sinha, Phys. Rev. D 88, (2013)] 17

18 Model Example The dominant decay mode to gauge boson inal states decays into particle via 3-body: g gg ~ ~ Since g ~ BR 10 3 produces dark matter at the end o the decay chain It is possible to have 3 body decay width larger than the 2-body decay width o moduli into gauginos [ g ~ g ~ is suppressed by (m gaugino /m ) 2 compared to gg ] Solves coincidence problem: BR B ~ BR ~

19 Model Examples: 2 can be a visible sector ield S (moduli is a hidden sector ield) W s hsx X 1 2 m S s 2 W=W s +W N,X m s ~ O(1) TeV, m X ~ O(10) TeV, m N ~ O(0.5) TeV BR ~ 10-6 Y s =(3/4)T r /m s ~ 10-4 n /s ~ S Decay + Annihilation or no annihilation works Allahverdi, Dutta, Sinha, Phys.Rev. D87 (2013)

20 Model Example 2 S Decay + Branching ratio Baryogenesis ~ 0.01 ~ 2 1 N1 2 O m 8 m X (10) or (m N1 /m X ) ~ 10-2 ~ 10-4 Y s =(3/4)T r /m s ~ 10-4 ~

21 Conclusion Understanding the origin o requires a connection between the particle physics and cosmology Non thermal dark matter can accommodate both over and under abundance scenarios Non-thermal scenarios can accommodate baryon abundance. Baryon abundance and dark matter abundance can be correlated---cladogenesis Small mass with -p ~ cm 2 can be accommodated with an explanation or the origin o n B ~n 21